Cosmic Microwave Background Anisotropy Measurement from Python V
We analyze observations of the microwave sky made with the Python experiment in its fifth year of operation at the Amundsen-Scott South Pole Station in Antarctica. After modeling the noise and constructing a map, we extract the cosmic signal from the data. We simultaneously estimate the angular powe...
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Online Access: | https://doi.org/10.1086/345714 |
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ftcaltechauth:oai:authors.library.caltech.edu:44daw-3vq37 2024-06-23T07:45:29+00:00 Cosmic Microwave Background Anisotropy Measurement from Python V Coble, K. Dodelson, S. Dragovan, M. Ganga, K. Knox, L. Kovac, J. Ratra, B. Souradeep, T. 2003-02-20 https://doi.org/10.1086/345714 unknown American Astronomical Society http://arxiv.org/abs/astro-ph/0112506 https://doi.org/10.1086/345714 oai:authors.library.caltech.edu:44daw-3vq37 eprintid:76009 resolverid:CaltechAUTHORS:20170408-144740114 info:eu-repo/semantics/openAccess Other Astrophysical Journal, 584(2), (2003-02-20) cosmic microwave background cosmology: observations info:eu-repo/semantics/article 2003 ftcaltechauth https://doi.org/10.1086/345714 2024-06-12T03:36:25Z We analyze observations of the microwave sky made with the Python experiment in its fifth year of operation at the Amundsen-Scott South Pole Station in Antarctica. After modeling the noise and constructing a map, we extract the cosmic signal from the data. We simultaneously estimate the angular power spectrum in eight bands ranging from large (ℓ ~ 40) to small (ℓ ~ 260) angular scales, with power detected in the first six bands. There is a significant rise in the power spectrum from large to smaller (ℓ ~ 200) scales, consistent with that expected from acoustic oscillations in the early universe. We compare this Python V map to a map made from data taken in the third year of Python. Python III observations were made at a frequency of 90 GHz and covered a subset of the region of the sky covered by Python V observations, which were made at 40 GHz. Good agreement is obtained both visually (with a filtered version of the map) and via a likelihood ratio test. © 2003. The American Astronomical Society. Received 2001 December 20; accepted 2002 October 22. This work was supported by the James S. McDonnell Foundation, PYI grant NSF AST 90-57089, and the NSF under a cooperative agreement with the Center for Astrophysical Research in Antarctica (CARA), grant NSF OPP 89-20223. CARA is an NSF Science and Technology Center. K. C. is supported by NSF grant AST 01-04465. The work of S. D. was supported by the DOE and by NASA grant NAG 5-10842 at Fermilab and by NSF grant PHY-0079251 at Chicago. B. R. and T. S. acknowledge support from NSF CAREER grant AST 98-75031. Published - pdf Submitted - 0112506.pdf Article in Journal/Newspaper Amundsen-Scott Antarc* Antarctica South pole South pole Caltech Authors (California Institute of Technology) Amundsen Scott South Pole Station ENVELOPE(0.000,0.000,-90.000,-90.000) Amundsen-Scott ENVELOPE(0.000,0.000,-90.000,-90.000) Amundsen-Scott South Pole Station ENVELOPE(139.273,139.273,-89.998,-89.998) Cara ENVELOPE(161.100,161.100,-82.750,-82.750) South Pole The Astrophysical Journal 584 2 585 592 |
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Caltech Authors (California Institute of Technology) |
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topic |
cosmic microwave background cosmology: observations |
spellingShingle |
cosmic microwave background cosmology: observations Coble, K. Dodelson, S. Dragovan, M. Ganga, K. Knox, L. Kovac, J. Ratra, B. Souradeep, T. Cosmic Microwave Background Anisotropy Measurement from Python V |
topic_facet |
cosmic microwave background cosmology: observations |
description |
We analyze observations of the microwave sky made with the Python experiment in its fifth year of operation at the Amundsen-Scott South Pole Station in Antarctica. After modeling the noise and constructing a map, we extract the cosmic signal from the data. We simultaneously estimate the angular power spectrum in eight bands ranging from large (ℓ ~ 40) to small (ℓ ~ 260) angular scales, with power detected in the first six bands. There is a significant rise in the power spectrum from large to smaller (ℓ ~ 200) scales, consistent with that expected from acoustic oscillations in the early universe. We compare this Python V map to a map made from data taken in the third year of Python. Python III observations were made at a frequency of 90 GHz and covered a subset of the region of the sky covered by Python V observations, which were made at 40 GHz. Good agreement is obtained both visually (with a filtered version of the map) and via a likelihood ratio test. © 2003. The American Astronomical Society. Received 2001 December 20; accepted 2002 October 22. This work was supported by the James S. McDonnell Foundation, PYI grant NSF AST 90-57089, and the NSF under a cooperative agreement with the Center for Astrophysical Research in Antarctica (CARA), grant NSF OPP 89-20223. CARA is an NSF Science and Technology Center. K. C. is supported by NSF grant AST 01-04465. The work of S. D. was supported by the DOE and by NASA grant NAG 5-10842 at Fermilab and by NSF grant PHY-0079251 at Chicago. B. R. and T. S. acknowledge support from NSF CAREER grant AST 98-75031. Published - pdf Submitted - 0112506.pdf |
format |
Article in Journal/Newspaper |
author |
Coble, K. Dodelson, S. Dragovan, M. Ganga, K. Knox, L. Kovac, J. Ratra, B. Souradeep, T. |
author_facet |
Coble, K. Dodelson, S. Dragovan, M. Ganga, K. Knox, L. Kovac, J. Ratra, B. Souradeep, T. |
author_sort |
Coble, K. |
title |
Cosmic Microwave Background Anisotropy Measurement from Python V |
title_short |
Cosmic Microwave Background Anisotropy Measurement from Python V |
title_full |
Cosmic Microwave Background Anisotropy Measurement from Python V |
title_fullStr |
Cosmic Microwave Background Anisotropy Measurement from Python V |
title_full_unstemmed |
Cosmic Microwave Background Anisotropy Measurement from Python V |
title_sort |
cosmic microwave background anisotropy measurement from python v |
publisher |
American Astronomical Society |
publishDate |
2003 |
url |
https://doi.org/10.1086/345714 |
long_lat |
ENVELOPE(0.000,0.000,-90.000,-90.000) ENVELOPE(0.000,0.000,-90.000,-90.000) ENVELOPE(139.273,139.273,-89.998,-89.998) ENVELOPE(161.100,161.100,-82.750,-82.750) |
geographic |
Amundsen Scott South Pole Station Amundsen-Scott Amundsen-Scott South Pole Station Cara South Pole |
geographic_facet |
Amundsen Scott South Pole Station Amundsen-Scott Amundsen-Scott South Pole Station Cara South Pole |
genre |
Amundsen-Scott Antarc* Antarctica South pole South pole |
genre_facet |
Amundsen-Scott Antarc* Antarctica South pole South pole |
op_source |
Astrophysical Journal, 584(2), (2003-02-20) |
op_relation |
http://arxiv.org/abs/astro-ph/0112506 https://doi.org/10.1086/345714 oai:authors.library.caltech.edu:44daw-3vq37 eprintid:76009 resolverid:CaltechAUTHORS:20170408-144740114 |
op_rights |
info:eu-repo/semantics/openAccess Other |
op_doi |
https://doi.org/10.1086/345714 |
container_title |
The Astrophysical Journal |
container_volume |
584 |
container_issue |
2 |
container_start_page |
585 |
op_container_end_page |
592 |
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1802639934867111936 |